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Project Cyclops, A Design... - Department of Earth and Planetary ...

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lO II<br />

Substituting this relation into equation 5, Chapter 5,<br />

with Po = fiB we find the conventional range limit<br />

o<br />

t---<br />

iv.<br />

10 to<br />

w 109<br />

._1<br />

R<br />

- 4 _'-B I (9)<br />

q__ dr t1_)1/2 n I]4, n >> I (10)<br />

m<br />

er<br />

u_ 108<br />

0<br />

¢Y<br />

w<br />

en<br />

z<br />

107<br />

where<br />

dr = receiving antenna diameter<br />

Peff = Ptgt = effective radiated power<br />

= noise spectral density = kTat radio frequencies<br />

B = receiver b<strong>and</strong>width<br />

10 6<br />

I01<br />

10 2 I0 3 I0 4 I0 5<br />

ANTENNA<br />

DIAMETER<br />

r = integration time<br />

n = (Br)<br />

Figure 6-4.<br />

Number <strong>of</strong> resolvable directions versus<br />

diameter<br />

SEARCH RANGE LIMIT<br />

<strong>and</strong> wavelength.<br />

in radio astronomy <strong>and</strong> in most fields <strong>of</strong> measurement<br />

the minimum detectable signal amplitude is defined<br />

as being equal to the rms fluctuations due to noise.<br />

The signal-to-noise power ratio out <strong>of</strong> a square-law<br />

detector is given by equation (19) in Chapter 5 as<br />

where<br />

Pr = received signal power<br />

Po = noise power<br />

s ('°r/t'o)2<br />

--= n (7)<br />

N 1 + 2(Pr/Po)<br />

n = (Br) = number <strong>of</strong> independent samples that<br />

are averaged<br />

Setting SIN equal to unity we find for the received<br />

signal-to-noise<br />

ratio<br />

Pr 1 +x/rl-+ n<br />

-- = (8)<br />

Po<br />

n<br />

We use equation (119) in estimating range limits when<br />

the data processing system is unspecified. However, in<br />

determining the performance <strong>of</strong> the <strong>Cyclops</strong> system we<br />

use the actual range limit at which the probability <strong>of</strong><br />

missing the signal Pros <strong>and</strong> the probability <strong>of</strong> a false<br />

alarm Pfa have specified values. That is, we take<br />

draper f -- q ,/2<br />

R = -- f(n,Pms,Pr,) I (11)<br />

4_--_<br />

where f(n,Pms,Pfq) is evaluated for the proposed data<br />

processing method using the actual statistics, <strong>and</strong> will be<br />

a number on the order <strong>of</strong> unity. Anticipating this, we<br />

will use as a reference range limit for some <strong>of</strong> our curves<br />

the range Ro<br />

given by<br />

/ \I/2<br />

dr(Peff.<br />

4\/<br />

which is simply the range at which the received<br />

signal-to-noise ratio is unity <strong>and</strong> is less than R, as given<br />

by equation (9), for n > 3.<br />

DOPPLER SHIFTS AND RATES<br />

Relative motion between transmitter <strong>and</strong> receiver can<br />

occur because <strong>of</strong> (1) radial velocity <strong>of</strong> the star with respect<br />

to the Sun, (2) orbital velocity <strong>of</strong> the <strong>Earth</strong> <strong>and</strong><br />

I<br />

56

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